There are 55 pulsars in the sample with \(\dot{E}>10^{35}\)  erg s\(^{-1}\) , only 5 of which are in the non-RVM class. A high fraction of these pulsars are seen at X-ray and/or \(\gamma \) -ray energies. In the outer-gap or two-pole caustic model of \(\gamma \) -ray emission [1]}, [2]} the expectation is that these pulsars are predominantly seen at high values of \(\alpha \) . In addition if \(\alpha \)  is randomly distributed at birth, then geometrical considerations again imply that high values of \(\alpha \)  should dominate in the observed population. However, a comprehensive study of these pulsars by [3]}, [4]} showed that either the \(\alpha \)  distribution is skewed towards low values or emission must arise from an open field-line region which is larger than conventionally defined from equation REF .
